DE CVn: A Bright, Eclipsing Red Dwarf -- White Dwarf Binary

Details DE CVn: A Bright, Eclipsing Red Dwarf -- White Dwarf Binary DE CVn: A Bright, Eclipsing Red Dwarf -- White Dwarf Binary

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007iaus..240..105v&link_type=abstract

Binary Stars as Critical Tools & Tests in Contemporary Astrophysics, Proceedings of IAU Symposium #240, held 22-25 August, 2006

Astronomy and Astrophysics

Astrophysics

Scientific paper

DE CVn is a relatively unstudied eclipsing binary where one of the components is an M dwarf. Its brightness makes it an ideal system for a detailed study in the context of common-envelope evolution of a detached white dwarf - red dwarf binary with a relatively short orbital period (8.7 hours). We present a detailed study of the basic parameters (e.g. orbital period, components' masses, spectral type) for this system from photometric and spectroscopic studies. The eclipses observed during several photometric observing runs were used to derive the ephemeris. We have used spectroscopic data to derive the radial velocity variations of the emission lines and these are used to determine the components' masses and the orbital separation. The secondary component in DE CVn is an M3 main-sequence star and the primary star, which is not visible in the spectra, is a cool white dwarf with a temperature of ˜8000 K. From the photometry and spectroscopy together, we have set a limit on the binary inclination. This system is a post-common-envelope system where the progenitor of the present day white dwarf was a low-mass star (M<2 Msun). The time before DE CVn becomes a semi-detached system is longer than the Hubble time.

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